Backscattering from the upper atmosphere /75-160 km/ detected by optical radar.
Ruby laser optical radar detection of upper atmospheric backscattering
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Ruby laser optical radar detection of upper atmospheric backscattering
Detection of the optical echoes from atmospheric constituents in the upper regions by optical radar
Optical radar experiments and meteoric fragmentation
Optical radar investigations of atmosphere, and Mie scattering intensity functions for backscatter
Optical radar studies of lower atmosphere, giving Mie theory calculations of clear atmosphere volume backscattering cross sections for four laser wavelengths
Optical radar system using corner reflector on lunar surface
Atmospheric optical radar Mie scattering
Detection of scattering layers in upper atmosphere by optical radar
The development of optical, radar, and candidate subsystems for Project Apollo is discussed. The design and development of the optical subsystems for both the Apollo command and lunar spacecraft are described. Design approaches, problems, and solutions are presented. The evolution of radar interfaces with the GN&C system is discussed; these interfaces involved both hardware and software in a relatively complex interrelationship. The design and development of three candidate subsystems are also described. The systems were considered for use in Apollo, but were not incorporated into the final GN&C system. The three subsystems discussed are the star tracker-horizon photometer, the map and data viewer and the lunar module optical rendezvous system.
80 km atmospheric backscattering enhancement detected by optical radar
An optical radar for detecting targets in natural waters was built and tested in the Gulf of Mexico. The transmitter consists of a Q switched neodymium glass laser, with output amplified and doubled in KDP to 0.53 micrometer wavelength. The receiver incorporates a noval optical spatial filter to reduce the dynamic range required of the photodetector to a reasonable value. Detection of targets to a depth of 26 meters (84 feet) was achieved with a considerable sensitivity margin. The sensitivity of the radar is highly dependent on the optical attenuation coefficient. In general, measured returns fell between the values predicted on the basis of monopath and multipath attenuation. By means of simple physical arguments, a radar equation for the system was derived. To validate this theoretical model, measurements of optical attenuation and of water surface behavior were also instrumented, and some of these results are given.
Optical radar detection of backscatter from upper atmosphere
Optical radar measurement of backscattering from mesopause region during July and August 1967
Upper atmospheric dust investigations using optical radar techniques
Aerosol content of mesosphere with noctilucent clouds measured with optical radar in Norway
The Jet Propulsion Laboratory has developed a set of computer programs known as the Solar System Data Processing System (SSDPS) which is employed in improving the ephemerides of the major planets and for improving the values of several associated astronomical constants. A group of solutions for the masses of the major planets, together with the AU and radii of Mercury, Venus, and Mars, is presented. These solutions based upon optical, radar, and spacecraft radio tracking data are preliminary. The relative power of radar and radio tracking data vis-a-vis purely optical data in a solution is shown. The problems which could arise by adopting solutions based upon a single data type are demonstrated.
The system is composed of an optical cavity with a laser and a mode locking means to build up an optical pulse. An optical switch is also provided within the cavity to convert the polarization of the optical pulse generated within the cavity. The optical switch comprises an electro-optical crystal driven by a time delayed driver circuit which is triggered by a coincident signal made from an optical pulse signal and a gating pulse signal. The converted optical pulse strikes a polarization sensitive prism and is deflected out of the cavity toward the pending target in the form of a pulse containing most of the optical energy generated by the laser in the pulse build-up period. After striking the target, the reflected energy is picked up by a transceiver with the total travel time of the pulse being recorded.
Lunar corner reflector landing proposal for laser beam precision measurements including Moon orbit, size, ephemeris time and libration